Horndeski and DHOST theories have been widely studied in cosmology (see for a nice review and references therein [1]}). Interestingly, in those theories the screening mechanism turns out to be partially broken in the case of astrophysical objects [2]}, such that the weak field equations are modified by the presence of terms with a numerical parameter, which encodes the information about the scalar field. This allows thus to study deviations from the Newtonian model of gravity, which is widely used to describe stellar and substellar objects. Similarly like other modified theories of gravity, the Poisson and hydrostatic equilibrium equations in such theories acquire additional terms (see [3]}, [4]}, [5]}; for review, [6]}, [7]}, [8]}). Because of that, there have been a few studies undertaken which demonstrated that the Chandrasekhar mass for white dwarf stars [9]}, [10]}, [11]}, [12]}, [13]}, [14]}, [15]}, [16]} may differ in modified gravity; the same happens with the minimum masses for hydrogen and deuterium burning [17]}, [18]}, [19]}, [20]}, [21]}, as well as Jeans and opacity masses [22]}, [23]}. Apart from those, the evolutionary pictures of stars and planets are also distinct with respect to Newtonian gravity [24]}, [25]}, [26]}, [27]}, [28]}, [29]}, [30]}. Those theories also modify the light elements' abundances in atmospheres [31]} and internal structures of terrestrial planets [32]}, [33]}, [34]}.
